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COSMO 09
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500/1-001 - Main Auditorium (CERN)
Antonio Riotto,
Gia Dvali,
Gian Giudice,
John Ellis,
Julien Lesgourgues,
Mikhail Shaposhnikov,
Ruth Durrer
Description
New: link to
Cosmo10
(Tokyo, 27 September - 1 October 2010)
Inflation, convenor: Andrew Liddle
Dark matter, convenor: Marco Cirelli
Dark energy and modified gravity, convenor: Kazuya Koyama
CMB, LSS and cosmological parameters/models, convenor: Licia Verde
String cosmology, convenor: Jim Cline
Baryogenesis and leptogenesis, convenor: Mariano Quiros
This year's edition of the annual Cosmo International Conference on Particle Physics and Cosmology -- Cosmo09 -- will be hosted by the CERN Theory Group from Monday September 7 till Friday September 11, 2009. The conference will take place at CERN, Geneva (Switzerland).
The Cosmo series is one of the major venues of interaction between cosmologists and particle physicists. In the exciting LHC era, the Conference will be devoted to the modern interfaces between Fundamental and Phenomenological Particle Physics and Physical Cosmology and Astronomy.
The Conference will be followed by the CERN TH Institute "Particle Cosmology" which will take place from Monday September 14 till Friday September 18, 2009. The CERN-TH Institutes are visitor programs intended to bring together scientists with similar interests and to promote scientific collaborations. If you wish to participate, please register on the Institute web page.
Link to last editions: COSMO 07 (U. of Sussex), COSMO 08 (U. of Wisconsin)
List of plenary speakers:
Gianfranco Bertone,
Pierre Binetruy,
Francois Bouchet,
Juerg Diemand,
Jonathan Feng,
Gregory Gabadadze,
Francis Halzen,
Steen Hannestad,
Will Kinney,
Johannes Knapp,
Hiranya Peiris,
Will Percival,
Syksy Rasanen,
Alexandre Refregier,
Pierre Salati,
Roman Scoccimarro,
Michael Schubnell,
Christian Spiering,
Neil Spooner,
Andrew Tolley,
Matteo Viel.
The plenary program is available on-line. Select "Preliminary programme" in the left menu and click on each plenary session to see details.
Parallel sessions:
The submission of talk proposals is closed by now. The parallel session program is available on-line. Select "Preliminary programme" in the left menu and click on each parallel session title to see details.
Posters. Participants willing to present a poster will be offered the opportunity to hang it in the hall, next to the main auditorium. The poster application is closed by now. The poster list is available on-line.
Registration.
On-line registration is open from January 16 till August 31 (click on the link in the left menu). There will be no registration fees.
[Thanks to the generosity of EU's network "UniverseNet", we have some limited funds available for supporting the visit of a few
young scientists who could not attend otherwise.
The application for funding is closed by now. All applicants have already been informed of the success of their application.]
Accomodation. Participants are expected to arrange their accomodation by themselves:
- some rooms with shower, wc and washbasin have been blocked in the CERN hostel for the conference (price: 58CHF/night). Unfortunately, all these rooms have already been booked.
- You can book a hotel in Geneva or in the area surrounding CERN using this list. If you book a hotel on the French side, be sure to have a passport or a visa valid also in France.
All participants are expected to be in possession of a passport or a visa valid in Swizerland (if relevant), and to be covered by their own health insurance during their visit.
Sponsors. This conference is receiving support from the European Community's Marie Curie Research and Training Network UniverseNet.
Support
Participants
348
View full list
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1
Welcome address and practical information
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10:45 AM
Coffea break
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Dark Energy and Modified Gravity 500/1-001 - Main Auditorium
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4:15 PM
Break
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Testing General Relativity on Cosmological Scales with Weak Gravitational LensingSpeaker: Ali VANDERVELD (Caltech/JPL)
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Dark Matter TH Theory Conference Room
TH Theory Conference Room
CERN
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Indirect Dark Matter searches with the PAMELA experiment: a wide range cosmic ray observatoryThe PAMELA apparatus has been launched in space on June 15, 2006 on the Russian Resurs DK1 satellite, and is continuously taking data since July 2006. The experiment is devoted to the precise and extensive measurements of cosmic ray in space, with main focus on the antiprotons and positrons in the 100 MeV/200 GeV energy range. Primary protons, electrons and light nuclei spectra are also precisely measured, and many solar physics and geomagnetic related aspects can be investigated with high statistics and long time exposure. This talk will present the latest analysis of the PAMELA data, with particular emphasis on the antiproton/proton and positron/electron ratio.Speaker: Oscar ADRIANI (Universita' di Firenze and INFN Firenze)
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Indirect dark matter searches with imaging atmospheric Cherenkov telescopesWIMPs annihilations produce very high energy gamma-rays in the final state. These gamma-rays may be detected by imaging atmospheric Cherenkov telescopes. Amongst the plausible targets are the Galactic Center, the center of galaxy clusters, dwarf Sphreroidal galaxies and substructures in Galactic haloes. Recent results from observations of ongoing IACTs will be presented. Constraints on the velocity-weighted annihilation cross section of Dark Matter particles are derived in the framework of models beyond the Standard Model of Particle Physics.Speaker: Emmanuel MOULIN (CEA Saclay, Irfu)
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Motivations for a New Force in the Dark SectorA new force in the dark sector, with GeV-scale force carriers, can change the expected properties of SUSY WIMP dark matter in significant ways. The annihilation cross section at low velocities is boosted by a Sommerfeld enhancement, perhaps by 2 or 3 orders of magnitude; the WIMP annihilates to the new force carrier, which immediately decays to light particles, bypassing constraints from antiprotons and pi-0 gammas; and excited states for the WIMP are naturally generated, making inelastic scattering possible. These are exactly the properties needed to explain recent results from cosmic ray measurements and the DAMA direct detection experiment, without violating the many tight constraints from other experiments. I will review the current status of the data, show how it can be explained with such a WIMP, and discuss the signals expected in future data sets.Speaker: Tracy SLATYER (Harvard University)
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Cosmic Rays from Dark Matter DecayA series of experiments measuring high-energy cosmic rays have recently reported strong indications for the existence of an exotic source of high-energy electrons and positrons. If interpreted in terms of the decay of dark matter particles, the PAMELA measurements of the positron fraction and the Fermi LAT measurements of the total electron plus positron flux restrict the possible decaying dark matter scenarios to a few cases. Pursuing a model-independent approach, we identify some promising scenarios of dark matter decay and calculate the predictions for the diffuse extragalactic gamma-ray flux, including the contributions from inverse Compton scattering with the interstellar radiation field.Speaker: David TRAN (Technical University of Munich)
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Galactic evolution and dark matter stabilityIf the dark matter sector in the universe is composed by metastable particles, galaxies and galaxy clusters are expected to undergo significant evolution from high to low redshift. We show that the decay of dark matter, with a lifetime compatible with cosmological constraints, can be at the origin of the observed evolution of the Tully-Fisher relation of disk galaxies and alleviate the problem of the size-evolution of elliptical galaxies.Speaker: Francesc FERRER (Washington University in St Louis)
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Constraints on annihilating Dark Matter from reionization and extragalactic gamma backgroundThe PAMELA, Fermi and HESS experiments (PFH) have shown anomalous excesses in the cosmic positron and electron fluxes. An exciting possibility is that the excesses arises due to annihilating Dark Matter (DM) particles with mass above 700 GeV. We calculate constraints on leptonically annihilating DM using the data of diffuse extragalactic gamma-ray background (EGR) and measurements of the optical depth (OD) to the last-scattering surface. We find that the constraints from OD are able to rule out the PFH favored region fully for the tau channel and almost fully for the \mu channel. Those constraints are quite robust with almost no dependence on low redshift DM clustering boost. The constraints from EGR are sensitive to the assumed halo concentration model and, for the power law model, rule out the PFH favored region for all leptonic annihilation channels. We also find that it is possible to have models that fully ionize the Universe at low redshifts. However, those models produce too large free electron fractions at z > ~100 and are in conflict with OD. Finally, we discuss about the motivation and the constraints for a more sophisticated annihilation scenario, where DM particles annihilate to intermediate metastable particles, which then decays to lepton pairs.Speaker: Andi HEKTOR (NICPB, Tallin)
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Constraints on Dark Matter models with large annihilation cross sections from the Early UniverseI will show how is it possible to place stringent constraints on high DM self-annihilation cross sections making use of cosmological observables. Current CMB measurements do in fact allow the possibility to limit down to the thermal values for particle masses of few GeV, with constraints that depend only on cosmological paramaters, and are not affected by astrophysical uncertainties. It is also possible to place strong constraints on self--annihilation cross sections by using observations related to the Epoch of Reionization, relying in this case on structure formation scenarios.Speaker: Fabio IOCCO (IPhT at CEA/Saclay; IAP Paris)
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4:00 PM
Break
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The Constrained NMSSM in the light of a bayesian analysisWe perform a global exploration of the Constrained Next to Minimal Supersymmetric Standard Model (CNMSSM) using Bayesian statistics. We present an analysis of several observables including collider signatures and predictions for direct detection of dark Matter.Speaker: Daniel LOPEZ-FOGLIANI (University of Sheffield)
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Scalar Dark Matter from Inert Doublet ModelThe Inert Doublet Model (IDM) provide a rather simple and yet rich extension of the Standard Model for Dark Matter. The dark matter candidate is the lightest neutral scalar of an extra SU(2)_L doublet which is odd under an unbroken Z2 symmetry. It can account for WMAP dark matter for 3 very different mass regimes: the low mass regime with m_dm~10, the middle mass regime with m_dm~m_W, and the high mass regime m_dm>500 GeV. In my talk I would like to address the richness of the phenomenology of the IDM and I will show how the constraints and the prospects for detection can vary with the mass range of interest.Speaker: Laura LOPEZ-HONOREZ (Universidad Autonoma de Madrid)
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Sterile neutrinos as dark matterThe discovery of neutrino masses suggests that the Standard Model should be supplemented with new gauge-singlet fermions, the sterile neutrinos. The number and the mass of sterile neutrinos are still undetermined. If one of these fermions has mass of several keV, it can account for the dark matter. Their relic abundance can be produced by several mechanisms. Different mechanisms result to "warmer" or "colder" dark matter that can explain the small-scale structure of the universe. If relic sterile neutrinos originate primarily from the decay of a scalar field at the electroweak scale, the resulting dark matter is much colder that the one produced in neutrino oscillations. This scalar field can be part of an extended Higgs sector, in which case it can also provide for a 1st order electroweak phase transition and yield observable signatures for accelerator experiments. The sterile-neutrino dark matter itself provides a potentially detectable signature from its two-body decay. The spectral line can be detected by X-ray telescopes. The same X-rays can speed up the formation of the first stars. A keV sterile neutrino can also give rise to the observed velocities of pulsars.Speaker: Kalliopi PETRAKI (UCLA)
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DAMA/LIBRA and leptonically interacting Dark MatterThe hypothesis that DM has tree-level interactions only with leptons has been proposed as an explanation for the annually modulated scintillation signal in DAMA/LIBRA versus the absence of a signal for nuclear recoils in experiments like CDMS or XENON10. I show that even in such a leptophilic DM scenario there are loop induced DM-nucleus interactions which dominate over DM-electron scattering. In the case of pseudoscalar or axial vector coupling between DM and leptons, where the loop diagrams vanish, the explanation of the DAMA signal in terms of DM-electron scattering is strongly disfavored by the spectral shape of the signal. Furthermore, if DM can annihilate into neutrinos or tau leptons, the required cross sections are excluded by many orders of magnitude using the Super-Kamiokande bound on neutrinos from DM annihilations in the Sun.Speaker: Thomas SCHWETZ (Max-Planck-Institute)
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A novel determination of the local dark matter densityWe present a novel study on the problem of constructing mass models for the Milky Way, concentrating on features regarding the dark matter halo component. We have considered a variegated sample of dynamical observables for the Galaxy, including several results which have appeared recently, and studied a 7- or 8-dimensional parameter space - defining the Galaxy model - by implementing a Bayesian approach to the parameter estimation based on a Markov Chain Monte Carlo method. The main result of this analysis is a novel determination of the local dark matter halo density which, assuming spherical symmetry and either an Einasto or an NFW density profile is found to be around 0.39 GeV cm^-3 with a 1-sigma error bar of about 7%; more precisely we find a rho_DM (R_0) = 0.385 \pm 0.027 GeV cm^-3 for the Einasto profile and rho_DM (R_0) = 0.389 \pm 0.025 GeV cm^-3 for the NFW. This is in contrast to the standard assumption that rho_DM (R_0) is about 0.3 GeV cm^-3 with an uncertainty of a factor of 2 to 3. A very precise determination of the local halo density is very important for interpreting direct dark matter detection experiments. Indeed the results we produced, together with the recent accurate determination of the local circular velocity, should be very useful to considerably narrow astrophysical uncertainties on direct dark matter detection.Speaker: Riccardo CATENA (SISSA)
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Dark Stars- Dark Matter and shaping the first StarsWe have proposed that the first phase of stellar evolution in the history of the Universe may be Dark Stars (DS), powered by dark matter heating rather than by nuclear fusion. The power source is annihilation of Weakly Interacting Massive Particles (WIMPs). These WIMPs are among the best motivated dark matter (DM) candidates and may be discovered by ongoing direct or indirect detection searches (e.g. FERMI /GLAST) or at the Large Hadron Collider at CERN. Dark stars look dramatically different from first stars without DM heating and can last from million to billions of years. Hence, DS should be observationally distinct from standard Pop III stars.Speaker: Douglas SPOLYAR (Fermi Lab)
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Higgs in Space!We consider the possibility that the Higgs can be produced in space in dark matter annihilations and its mass determined by measuring the spectrum of gamma ray lines. We provide a simple class of models where the dark matter is a Dirac fermion that couples to a new Z' that dominantly annihilates into top quarks. The class of models under consideration turns out to arise naturally in the context of Randall--Sundrum models and more generally in models where the top quark has strong couplings with the dark sector.Speaker: Marco TAOSO (University of Padova)
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Reception Main building
Main building
CERN
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10:45 AM
Coffea break
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CMB, LSS, cosmological models and parameters 500/1-001 - Main Auditorium
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Two-minute presentations of selected postersSpeakers: Martins, bonvin
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3:55 PM
Break
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Two-minute presentations of selected postersSpeakers: D'Amico, Fauvet, Fraisse
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String Cosmology TH Theory Conference Room
TH Theory Conference Room
CERN
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Non-local cosmological models from String Field Theorycosmological models from String Field Theory In this talk I'm going to review the recent activity on cosmological models involving a non-local scalar field motivated by the String Field Theory focusing on the mathematical aspects and applications to the Dark Energy problem. Models of this type exhibit new interesting properties compared to models with local fields. Exact solutions and behavior of perturbations are presented. Cosmological applications and restrictions coming from the observational data are emphasized. Field theoretical aspects of such non-local models are discussed. Mainly based on: Alexey S. Koshelev, work in progress; Alexey S. Koshelev, Sergey Yu. Vernov, ``Cosmological perturbations in SFT inspired non-local scalar field models'', arXiv:0903.5176; I. Ya. Aref'eva, A. S. Koshelev, ``Cosmological Signature of Tachyon Condensation'', JHEP \textbf{0809} (2008) 068, arXiv:0804.3570; Alexey S. Koshelev, ``Non-local SFT Tachyon and Cosmology'', JHEP \textbf{0704} (2007) 029, hep-th/0701103.Speaker: Alexey KOSHELEV
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Gaugino condensation in the early universeSpeaker: Marieke Postma
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Circumventing the Eta problemSpeaker: Ruth Gregory
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Combined local and equilateral non-Gaussianities in multifield DBI inflationSpeaker: Sebastien Renaux-Petel
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Brane inflation and the overshoot problemSpeaker: Simeon Bird
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Alleviating the Fine-Tuning of Brane-Antibrane Inflation ModelsSpeaker: Loison Hoi
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4:10 PM
Break
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Strings across Kasner singularitiesSpeaker: Gustavo Niz
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Curvatons in Warped ThroatsSpeaker: Takeshi Kobayashi
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Cosmological Fluctuations From Infra-Red Cascading During InflationSpeaker: Neil Barnaby
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Gravitational waves from broken cosmic superstrings: The bursts and the BeadsSpeaker: Benjamin Shlaer
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On the full trispectrum in multi-field DBI inflationSpeaker: Shuntaro Mizuno
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11:15 AM
Coffee break
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CERN Colloquium by Pr. Steven Hawking 500/1-001 - Main Auditorium
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Social event: Attribution of the Tomalla Prize 2009 for gravity research to Viatcheslav Mukhanov and Alexei Starobinsky at Geneva University (ceremony, talks, aperitif) Geneva University (Geneva University)
Geneva University
Geneva University
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10:45 AM
Coffea break
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4:00 PM
Break
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6:00 PM
Session ends
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Particle physics in the early universe TH Theory Conference Room
TH Theory Conference Room
CERN
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4:15 PM
Break
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10:30 AM
Coffea break
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Concluding remarks and COSMO'10 announcement
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